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- W2056553538 abstract "The energy distribution functions of nonthermal thermospheric hydrogen atoms are calculated for electron and proton precipitation in the Jovian aurora. A numerical model taking into account the production, elastic and inelastic relaxation and transport processes for hot H atoms is developed. This model is based on a Monte Carlo solution of the nonlinear Boltzmann equation for hot H atoms produced by electron and proton impact on H and H 2 and exothermic chemical reactions. The distribution functions show a much higher energy tail for proton than electron precipitation. It is shown that the steady state flux of hot atoms ( E ≥ 2 eV) is essentially isotropic. The peak and column hot H densities are about 3 × 10 5 cm −3 and 1 × 10 14 cm −3 for a 100 erg cm −2 s −1 precipitation combining hard (22 keV) and soft (0.2 keV) electrons mixed with a 10 erg cm −2 s −1 flux of soft (0.3 keV) protons. These column densities, coupled with the wide range of hot H atom energies, may play an important role in the formation of the Lyman α line profile. Multiple scattering in the wings of the Ly α line by the fast H atoms is shown to partly account for the broad Ly α profile observed in the Jovian aurora with the Hubble space telescope." @default.
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- W2056553538 date "1996-09-01" @default.
- W2056553538 modified "2023-09-27" @default.
- W2056553538 title "The distribution of hot hydrogen atoms produced by electron and proton precipitation in the Jovian aurora" @default.
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- W2056553538 doi "https://doi.org/10.1029/96je01952" @default.
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